Context. High-mass stars play a prominent role in Galactic evolution, but their formation mechanism is still poorly understood. This lack of knowledge reflects the observational limitations of present instruments, whose angular resolution (at the typical distances of massive protostars) precludes probing circumstellar gas on scales of 1–100 AU, relevant for a detailed investigation of accretion structures and launch/collimation mechanims of outflows in high-mass star formation.
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Moscadelli et al. (2011) studied this question.
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